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SUMMARY:Modelling solar eruptive events from their onset to their propagat
 ion at 1 AU
DTSTART;VALUE=DATE-TIME:20230510T101000Z
DTEND;VALUE=DATE-TIME:20230510T102500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115654Z
UID:indico-contribution-330@meetings.aip.de
DESCRIPTION:Speakers: Antoine Strugarek ()\nIn the era of Solar Orbiter an
 d Parker Solar Probe\, we have now an unprecedented view on eruptive event
 s of the Sun\, from their onset to their propagation in the heliosphere. T
 hanks to the proximity of the probes to the Sun for at least part of their
  orbit\, we are currently acquiring more and more key data on the structur
 ing and the propagation of solar eruptive events\, as well as on the accel
 eration of particles at each stage of the eruption and propagation.\n\nI w
 ill report on an on-going modelling effort of solar eruptive events using 
 the versatile PLUTO code within the STORMGENESIS project. I will present a
  full MHD effort to model idealised and realistic and eruptive active regi
 ons\, based on the initiation of the magnetic with both non-linear force-f
 ree and non force-free extrapolations. I will present very recent result o
 n the modelling of the eruption of active region #12241\, which is well re
 produced when using a non force-free initiation. Coupled to charged test-p
 articles under the gyrokinetic approximation\, and to the heating and cool
 ing associated with magnetic reconnection and radiative losses\, I will pr
 esent first results on the prediction for thermal and non-thermal emission
  from this active region. \n\nIn a second part\, I will show how the same 
 simulation framework\, now using adaptive mesh refinement\, can be used to
  model the propagation of coronal mass ejections from their onset to their
  propagation up to 1 AU in a realistically structured solar wind. These re
 sults\, published recently in Regnault et al. (2023)\, allow to highlight 
 the generic features of CMES and the simulation results compare very well 
 with superposed-epochs analysis of hundreds of CMEs. In addition\, these s
 imulations point towards various rotation patterns of the CMEs that depend
  on their size and that happen during the initial stage of their propagati
 on within the Alfvén surface. These results warrant further analyses\, co
 upling the two set of simulations presented here to provide a complete pic
 ture of the energetics and of thermal and non-thermal emission of solar er
 uptive events.\n\nhttps://meetings.aip.de/event/24/contributions/330/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/24/contributions/330/
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